Time Series Analysis with Clean - Part One - Derivation of a Spectrum

Roberts, D. H.; Lehár, Joseph; Dreher, J. W.

doi:10.1086/114383

Cited by 809 publications

(671 citation statements)

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“…The agreement between the two periods is excellent. These values are confirmed with the clean algorithm (Roberts et al 1987), which removes spurious periods caused by the window function. The Lomb-Scargle periodogram in a range of frequencies 0 -10 d −1 and an inset of the clean periodogram, up to ν = 5 d −1 are shown in Figure 4.…”

Section: Period Determinationsupporting

confidence: 61%

The massive multiple system HD 64315

Lorenzo

Negueruela

Vilardell

et al. 2017

A&A

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Context. The O6 Vn star HD 64315 is believed to belong to the star-forming region known as NGC 2467, but previous distance estimates do not support this association. Moreover, it has been identified as a spectroscopic binary, but existing data support contradictory values for its orbital period. Aims. We explore the multiple nature of this star with the aim of determining its distance, and understanding its connection to NGC 2467. Methods. A total of 52 high-resolution spectra have been gathered over a decade. We use their analysis, in combination with the photometric data from All Sky Automated Survey and Hipparcos catalogues, to conclude that HD 64315 is composed of at least two spectroscopic binaries, one of which is an eclipsing binary. We have developed our own program to fit four components to the combined line shapes. Once the four radial velocities were derived, we obtained a model to fit the radial-velocity curves using the Spectroscopic Binary Orbit Program (SBOP). We then implemented the radial velocities of the eclipsing binary and the light curves in the Wilson-Devinney code iteratively to derive stellar parameters for its components. We were also able to analyse the non-eclipsing binary, and to derive minimum masses for its components which dominate the system flux. Results. HD 64315 contains two binary systems, one of which is an eclipsing binary. The two binaries are separated by ∼ 0.09 arcsec (or ∼ 500 AU) if the most likely distance to the system, ∼ 5 kpc, is considered. The presence of fainter companions is not excluded by current observations. The non-eclipsing binary (HD 64315 AaAb) has a period of 2.70962901 ± 0.00000021 d. Its components are hotter than those of the eclipsing binary, and dominate the appearance of the system. The eclipsing binary (HD 64315 BaBb) has a shorter period of 1.0189569 ± 0.0000008 d. We derive masses of 14.6 ± 2.3 M ⊙ for both components of the BaBb system. They are almost identical; both stars are overfilling their respective Roche lobes, and share a common envelope in an overcontact configuration. The non-eclipsing binary is a detached system composed of two stars with spectral types around O6 V with minimum masses of 10.8 M ⊙ and 10.2 M ⊙ , and likely masses ≈ 30 M ⊙ . Conclusions. HD 64315 provides a cautionary tale about high-mass star isolation and multiplicity. Its total mass is likely above 90 M ⊙ , but it seems to have formed without an accompanying cluster. It contains one the most massive overcontact binaries known, a likely merger progenitor in a very wide multiple system.

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Section: Period Determinationsupporting

confidence: 61%

The massive multiple system HD 64315

Lorenzo

Negueruela

Vilardell

et al. 2017

A&A

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“…In addition, the standard deviation within each lightcurve as a function of the object brightness can be used to derive a second variability index. Sinusoidal signals are identified by a combination of the Scargle-Lomb periodogram (Scargle 1982) and the CLEAN algorithm (Roberts et al 1987). Identified binaries can be analysed using the DEBIL/MECI programs (Devor 2005 andDevor &Charbonneau 2006).…”

Section: Discussionmentioning

confidence: 99%

TEST The Tautenburg Exoplanet Search Telescope

Eigmüller

Eislöffel

2008

Proc. IAU

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Abstract. The Tautenburg Exoplanet Search Telescope (TEST) is a robotic telescope system. The telescope uses a folded Schmidt Camera with a 300mm main mirror. The focal length is 940mm and it gives a 2.2 • × 2.2 • field of view. Dome, mount, and CCD cameras are controlled by a software bundle made by Software Bisque. The automation of the telescope includes selection of the night observing program from a given framework, taking darks and skyflats, field identification, guiding, data taking, and archiving. For the search for transiting exoplanets and variable stars an automated psf photometry based on IRAF and a lightcurve analysis based on ESO-Midas are conducted. The images and the results are managed using a PostgreSQL database.

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“…The two next highest peaks (indicated with arrows) turn out to be 1 day aliases. To illustrate this, we have applied the CLEAN algorithm as implemented by Roberts et al (1987) to remove the effects of the window function. The second panel of Figure 5 shows that only the 0.837 day peak survives this process, suggesting that it is a real signal.…”

Section: Study Of the Light-curve Residualsmentioning

confidence: 99%

Absolute Properties of the Spotted Eclipsing Binary Star Cv Boötis

Torres

Vaz

Lacy

2008

The Astronomical Journal

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We present new V-band differential brightness measurements as well as new radial-velocity measurements of the detached, circular, 0.84 day period, double-lined eclipsing binary system, CV Boo. These data, along with other observations from the literature, are combined to derive improved absolute dimensions of the stars for the purpose of testing various aspects of theoretical modeling. Despite complications from intrinsic variability that we detect in the system, and despite the rapid rotation of the components, we are able to determine the absolute masses and radii to better than 1.3% and 2%, respectively. We obtain M A = 1.032 ± 0.013 M and R A = 1.262 ± 0.023 R for the hotter, larger, and more-massive primary (star A), and M B = 0.968 ± 0.012 M and R B = 1.173 ± 0.023 R for the secondary. The estimated effective temperatures are 5760 ± 150 K and 5670 ± 150 K, respectively. The intrinsic variability with a period ∼1% shorter than the orbital period is interpreted as being due to modulation by spots on one or both components. This implies that the spotted star(s) must be rotating faster than the synchronous rate, which disagrees with predictions from current tidal evolution models according to which both stars should be synchronized. We also find that the radius of the secondary is larger than expected from stellar evolution calculations by ∼10%, a discrepancy also seen in other (mostly lower-mass and active) eclipsing binaries. We estimate the age of the system to be approximately 9 Gyr. Both components are near the end of their main-sequence phase, and the primary may have started the shell hydrogen-burning stage.

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Time Series Analysis with Clean - Part One - Derivation of a Spectrum

Cited by 809 publications

References 0 publications

The massive multiple system HD 64315

The massive multiple system HD 64315

TEST The Tautenburg Exoplanet Search Telescope

Absolute Properties of the Spotted Eclipsing Binary Star Cv Boötis

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